Context : It has been speculated that WR winds may have contaminated the forming solar system , in particular with short-lived radionuclides ( half-lives in the approximate 10 ^ { 5 } -10 ^ { 8 } y range ) that are responsible for a class of isotopic anomalies found in some meteoritic materials .

Aims : We revisit the capability of the WR winds to eject these radionuclides using new models of single non-exploding WR stars with metallicity Z = 0.02 .

Methods : The earlier predictions for non-rotating WR stars are updated , and models for rotating such stars are used for the first time in this context .

Results : We find that ( 1 ) rotation has no significant influence on the short-lived radionuclide production by neutron capture during the core He-burning phase , and ( 2 ) { } ^ { 26 } \kern - 0.8 ptAl , { } ^ { 36 } \kern - 0.8 ptCl , { } ^ { 41 } \kern - 0.8 ptCa , and { } ^ { 107 } \kern - 0.8 ptPd can be wind-ejected by a variety of WR stars at relative levels that are compatible with the meteoritic analyses for a period of free decay of around 10 ^ { 5 } y between production and incorporation into the forming solar system solid bodies .

Conclusions : We confirm the previously published conclusions that the winds of WR stars have a radionuclide composition that can meet the necessary condition for them to be a possible contaminating agent of the forming solar system .
Still , it remains to be demonstrated from detailed models that this is a sufficient condition for these winds to have provided a level of pollution that is compatible with the observations .